Pulsation and Long-Term Variability of the High-Amplitude
                    <i>δ</i>
                    Scuti Star AD Canis Minoris

Khokhuntod, Pongsak; Fu, Jian-Ning; Boonyarak, Chayan; Marak, Kanokwan; Chen, Li; Jiang, Shi-Yang

doi:10.1088/1009-9271/7/3/12

Cited by 6 publications

(13 citation statements)

References 9 publications

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“…Our 700‐d long data set is in a good qualitative agreement with Laney et al (2002). The limits on the orbital period and RV amplitude suggest a binary companion of about 1 M ⊙ , possibly a white dwarf star. The radial velocity curve of AD CMi shows cycle‐to‐cycle variations that support the presence of a low‐frequency mode pulsation reported by Khokhuntod et al (2007). The centre‐of‐mass velocity is in a good agreement with the previous measurement by Balona & Stobie (1983) and does not contradict the binary hypothesis of the star, since the predicted γ‐velocity change is around 1 km s −1 . We obtained the first spectroscopic measurements for BE Lyn.…”

Section: Discussionsupporting

confidence: 89%

“…This might be due to the presence of an additional pulsation mode but our data are not extensive enough to resolve multiple modes. If this secondary mode is the same one reported by Khokhuntod et al (2007), its amplitude must change in time, because the very low amplitude in the Khokhuntod et al (2007) data is hardly compatible with the 2–3 km s −1 cycle‐to‐cycle RV change we find in the spectroscopic measurements. It is interesting to add that the Abhyankar (1959) data showed a larger peak‐to‐peak amplitude of about 35 km s −1 , which may also be due to cycle‐to‐cycle variations caused by a second excited mode.…”

Section: Resultsmentioning

confidence: 61%

“…They deduced the presence of light‐time effect due to binarity and a slow period increase due to evolutionary effect. In addition, Khokhuntod et al (2007) detected an extra low‐frequency component in the photometric data, which provides a possible explanation for the large scatter of the O–C diagram.…”

Section: Resultsmentioning

confidence: 86%

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Binarity and multiperiodicity in high-amplitude δ Scuti stars

Derekas

Kiss

Bedding

et al. 2009

Monthly Notices of the Royal Astronomical Society

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We have carried out a photometric and spectroscopic survey of bright high‐amplitude δ Scuti (HADS) stars. The aim was to detect binarity and multiperiodicity (or both) in order to explore the possibility of combining binary star astrophysics with stellar oscillations. Here, we present the first results for 10, predominantly southern, HADS variables. We detected the orbital motion of RS Gru with a semi‐amplitude of ∼6.5 km s−1 and 11.5 d period. The companion is inferred to be a low‐mass dwarf star in a close orbit around RS Gru. We found multiperiodicity in RY Lep from both photometric and radial velocity data and detected orbital motion in the radial velocities with hints of a possible period of 500–700 d. The data also revealed that the amplitude of the secondary frequency is variable on the time‐scale of a few years, whereas the dominant mode is stable. Radial velocities of AD CMi revealed cycle‐to‐cycle variations, which might be due to non‐radial pulsations. We confirmed the multiperiodic nature of BQ Ind, while we obtained the first radial velocity curves of ZZ Mic and BE Lyn. The radial velocity curve and the O–C diagram of CY Aqr are consistent with the long‐period binary hypothesis. We took new time series photometry on XX Cyg, DY Her and DY Peg, with which we updated their O–C diagrams.

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Section: Discussionsupporting

confidence: 89%

Section: Resultsmentioning

confidence: 61%

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Binarity and multiperiodicity in high-amplitude δ Scuti stars

Derekas

Kiss

Bedding

et al. 2009

Monthly Notices of the Royal Astronomical Society

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“…The newest research paper of this star was published by Khokhuntod et al (2007). The authors used presented 74 times of maximum light.…”

Section: Ad CMImentioning

confidence: 99%

“…Papers have been published about AD CMi (Khokhuntod et al 2007), DY Her (Boonyarak and Jiang 2007), KZ Hya (Fu et al 2008), DY Peg (Fu et al 2009), andVZ Cnc (Boonyarak et al 2009). In this paper we present (O-C) calculations for 14 HADS (GP And, CY Aqr, BS Aqr, YZ Boo, AD CMi, VZ Cnc, EH Lib, DY Her, V927 Her, KZ Hya, BE Lyn, V1162 Ori, DY Peg, and CW Ser) among our monitoring targets by using all times of light maximum available.…”

Section: Introductionmentioning

confidence: 99%

On the period variations of several low declination high amplitude delta Scuti variables

Boonyarak

Khokhuntod

et al. 2011

Astrophys Space Sci

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A 16-inch Schmidt-Cassegrain telescope on the campus of Naresuan University of Thailand and several similar-size telescopes in China equipped with CCD cameras were used to observe 14 high amplitude delta Scuti stars: GP And, CY Aqr, BS Aqr, YZ Boo, AD CMi, VZ Cnc, EH Lib, DY Her, V927 Her, KZ Hya, BE Lyn, V1162 Ori, DY Peg, and CW Ser, between the years 1999 and 2010. Data were also collected from scientific journals and sources on the Internet for these variable stars. Times of light maximum of these delta Scuti stars were then either determined from the observations or obtained from the literature to analyze the pulsation period variations. For the 14 delta Scuti stars we concluded that 7 stars (BS Aqr, CY Aqr, AD CMi, EH Lib, KZ Hya, BE Lyn and DY Peg) are binary or multiple systems. 10 delta Scuti stars are found with periods increasing with rates between 5.86 × 10 −9 and 2.34 × 10 −6 per year and the other 4 stars (BS Aqr, DY Her, BE Lyn and DY Peg) show periods decreasing with rates of about 10 −9 to 10 −8 per year.

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Variability Study of the SX Phoenicis Star BL Camelopardalis

Zhang

Marak

et al. 2008

Chin. J. Astron. Astrophys.

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Pulsation and Long-Term Variability of the High-Amplitude δ Scuti Star AD Canis Minoris

Cited by 6 publications

References 9 publications

Binarity and multiperiodicity in high-amplitude δ Scuti stars

Binarity and multiperiodicity in high-amplitude δ Scuti stars

On the period variations of several low declination high amplitude delta Scuti variables

Variability Study of the SX Phoenicis Star BL Camelopardalis

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